For a geometry given by \((f_{\mathrm {fill}},{R_{\textnormal {acc}}},{r_{\rm max}})\) , the main quantities defining the parameter space are
the mass accretion rate \(\dot{M} \) , the planet mass \(M_{\mathrm {p}}\) , and the planet radius \(R_{\mathrm {p}}\) .
We consider a range of accretion rates \(\dot{M} \approx 3\times 10^{-8}\) –\(3\times 10^{-4}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\) . The high end of the \(\dot{M} \)  range is higher than usually found in planet formation models [1]}, [2]} but could be relevant to an accretion outburst akin to the situation of FU Orionis stars [3]}.
With these high accretion rates, we can address whether we would indeed observe a signal in the (perhaps unlikely) event a planet were caught outbursting.
This range also covers the accretion rate inferred for the PDS 70 planets
[4]}, [5]}.
